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This paper presents the first systematic study of proto-neutron star (PNS)convection in three dimensions (3D) based on our latest numerical Fornax modelsof core-collapse supernova (CCSN). We confirm that PNS convection commonlyoccurs, and then quantify the basic physical characteristics of the convection.By virtue of the large number of long-term models, the diversity of PNSconvective behavior emerges. We find that the vigor of PNS convection is notcorrelated with CCSN dynamics at large radii, but rather with the mass of PNS$-$ heavier masses are associated with stronger PNS convection. We find thatPNS convection boosts the luminosities of $\nu_{\mu}$, $\nu_{\tau}$,$\bar{\nu}_{\mu}$, and $\bar{\nu}_{\tau}$ neutrinos, while the impact on otherspecies is complex due to a competition of factors. Finally, we assess theconsequent impact on CCSN dynamics and the potential for PNS convection togenerate pulsar magnetic fields.

A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations